A field theory approach to cosmological density perturbations

Adiabatic perturbations propagate in the expanding universe like scalar massless fields in some effective Robertson–Walker space–time.     

Evolution of nonlinear cosmological perturbations

We define fully nonperturbative generalizations of the uniform density and comoving curvature perturbations, which are known, in the linear theory, to be conserved on sufficiently large scales for adiabatic perturbations. Our nonlinear generalizations are defined geometrically, independently of any coordinate system. We give the equations governing their evolution on all scales. Also, in order to make contact with previous works on first- and second-order perturbations, we introduce a coordinate system and show that previous results can be recovered, on large scales, in a remarkably simple way, after restricting our definitions to first and second orders in a perturbative expansion.     

The cosmological constant of modular closed string field theory. I

We formulate closed string field theory as a quantum theory of modular geometry. We determine the full interacting quantum hamiltonian to all loop orders in perturbation theory. The free action has a new highly non-linear symmetry acting on the string field, and the kinetic operator. Perturbatively we demonstrate that the new theory gives the correct expression for the cosmological constant that is ultraviolet finite to one-loop order.     

Linear perturbations on the cosmological background in the relativistic theory of gravitation: I. Theory

We have derived a system of second-order ordinary differential equations to describe the evolution of small perturbations in the gravitational field and matter characteristics in RTG, with the cosmological solution being a background. These equations are shown to admit the effective gauge invariance, since the graviton mass can be neglected in most cases of interest. The standard expansion in scalar, vector, and tensor components is performed. The equations have been derived for each component.     

Linear perturbations on the cosmological background in the relativistic theory of gravitation: II. Appendix

We have solved the general equations derived in Part I [1] to describe the evolution of the gravitational instability on the background of an oscillating, homogeneous, and isotropic universe in the relativistic theory of gravitation considering a massive graviton. Complete solutions, along with their short-wave and long-wave asymptotics, are given for most distinctive stages of the evolution of the universe, namely, near the turning points corresponding to the maximum and minimum densities, as well as in the radiation-dominated, nonrelativistic, and quintessence stages. In all these cases, except for the turning points, the gauge vectors have been determined for the scalar and vector perturbations, allowing the elimination of wave solutions with a phase velocity that is equal to the speed of light. We conclude that, in principle, the observed structure of the universe could have been formed during a sufficiently large number of its cycles.     

Evolution of cosmological perturbations in a brane-universe

In our present Letter, we analyze the impact of the existence of extra dimensions on cosmology, in particular, on the evolution of cosmological perturbations. For a five-dimensional anti-de Sitter spacetime where ordinary matter is confined to a brane-universe, the equations governing the cosmological perturbations are presented in a form very close to the equations of standard cosmology. Two types of corrections appear: corrections due to the unconventional evolution of the homogeneous solution, which change the background-dependent coefficients of the equations, and corrections due to the curvature along the fifth dimension, which act as source terms in the evolution equations.     

Progressing wave perturbations of cosmological spacetimes

We determine the large class of Robertson-Walker spacetimes whose first-order, linear, isentropic perturbations can be expressed in closed form, and the closed form perturbations are written down. It is shown that the class includes several well-known spacetimes including, for example, spatially flat dust and the radiation filled universe.     

Gauge-invariant perturbations in anisotropie homogeneous cosmological models

In a recent paper K. Tomita and M. Den found a set of coupled differential equations for spatially flat, anisotropic homogeneous,N- dimensional cosmological models. Some particular exact solutions of those differential equations for a few specific equations of state were obtained by D. Lorentz-Petzold. In the present work we solve those differential equations completely.     

Density perturbations in a Brans-Dicke cosmological model

A very general flat solution for Brans-Dicke cosmology with a perfect-fluid, Robertson-Walker metric and a perfect gas law of state is examined regarding density perturbations. The model has growing instabilities, but not of exponential character.     

Integration theory of observables

Representations of abstract observables on a generalised logic are given in terms of bounded vector-valued Borel measures on the real line whose ranges are in the dual spaceX ^* of the Banach space of statesX. Each bounded observable is furthermore represented by an elementu ^* ofX ^* such that for any proper statep X, u ^* (p) is the expectation value ofu when the system is in the statep.     

Density perturbations in a cosmological de Donder gauge

Density perturbations are considered during the radiation-dominated and the dust-dominated periods of the expanding universe. The perturbations are taken to have spherical symmetry and the investigation is carried out in the de Donder gauge. In order to guarantee the energy-momentum conservation of the perturbation in the de Donder gauge a compatibility condition is obtained. Equations for the propagation of a spherically symmetric perturbation in linear approximation on a FRW cosmological background are presented. It turns out that the evolutiontendency of the formation is mainly predicted by the state of the cosmic background. A radiation-dominated universe does not stimulate growth processes; the perturbation will be in a frozen state or it will diffuse. It is found that the dust-dominated universe stimulates the perturbation mass to grow. The rate of this cosmic affected growing process is proportional toR ^–1 (R being the scale factor of the universe), so that it seems that almost all galaxies were formed at the beginning of the present dust-dominated era.